The recent theoretical study of [1]} also deals with the absorption of the flux from a planet by material in the system.
Our approaches are similar but distinct:
they use interstellar medium (ISM) dust opacity values (we attempt to estimate them specifically for accretion onto planets, and consider also absorption by the gas) to address the extinction in different infrared filters (we deal with one accretion line).
The flow geometry is handled differently (in 3D in their case, albeit with a non-zero smoothing length),
the parameter space is surveyed to a different extent (more broadly in our case, and with \(\dot{M}\)  and \(M_{\mathrm {p}}\)  independent), and the thermodynamics are treated differently (they assume isothermal gas, while we take the radiation transport into account), while the radiative transfer is similar in both.
Thus in many respects the study of [1]} and ours are complementary.
